STEREO quadrature observations of coronal dimming at the onset of mini-CMEs

Innes, D. E.; McIntosh, Scott W.; Pietarila, A.

doi:10.1051/0004-6361/201014366

Cited by 34 publications

(36 citation statements)

References 12 publications

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“…They are associated with the eruption that started along y = 170 at 07:20 UT (Fig. 3b) in which both prominence and corona take off simultaneously, similar to the mini-CME onsets reported by Innes et al (2010). The prominence, visible as a dark front, reached the SUMER slit at 07:29 UT.…”

Section: Ejecta Fronts and Oscillationssupporting

confidence: 77%

Oscillations in the wake of a flare blast wave

Tothova

Innes²,

Stenborg³

2011

A&A

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Context. Oscillations of coronal loops in the Sun have been reported in both imaging and spectral observations at the onset of flares. Images reveal transverse oscillations, whereas spectra detect line-of-sight velocity or Doppler-shift oscillations. The Doppler-shift oscillations are commonly interpreted as longitudinal modes. Aims. Our aim is to investigate the relationship between loop dynamics and flows seen in TRACE 195 Å images and Doppler shifts observed by SUMER in Si iii 1113.2 Å and Fe XIX 1118.1 Å at the time of a C.8-class limb flare and an associated CME. Methods. We carefully co-aligned the sequence of TRACE 195 Å images to structures seen in the SUMER Si iii, Ca X, and Fe XIX emission lines. Additionally, Hα observations of a lifting prominence associated with the flare and the coronal mass ejection (CME) are available in three bands around 6563.3 Å. They give constraints on the timing and geometry. Results. Large-scale Doppler-shift oscillations in Fe XIX and transverse oscillations in intensity images were observed over a large region of the corona after the passage of a wide bright extreme-ultraviolet (EUV) disturbance, which suggests ionization, heating, and acceleration of hot plasma in the wake of a blast wave.

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Section: Ejecta Fronts and Oscillationssupporting

confidence: 77%

Oscillations in the wake of a flare blast wave

Tothova

Innes²,

Stenborg³

2011

A&A

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“…The microflares and associated coronal dimmings in quiet regions are essentially the same as those observed in active regions (Innes et al 2009(Innes et al , 2010. Quiet regions are supposedly filled with closed magnetic fields (Ito et al 2010).…”

Section: Discussionmentioning

confidence: 55%

Evolution of microflares associated with bright points in coronal holes and in quiet regions

Kamio

Curdt

Teriaca

et al. 2011

A&A

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Aims. We aim to find similarities and differences between microflares at coronal bright points found in quiet regions and coronal holes, and to study their relationship with large scale flares. Methods. Coronal bright points in quiet regions and in coronal holes were observed with Hinode/EIS using the same sequence. Microflares associated with bright points are identified from the X-ray lightcurve. The temporal variation of physical properties was traced in the course of microflares.Results. The lightcurves of microflares indicated an impulsive peak at hot emission followed by an enhancement at cool emission, which is compatible with the cooling model of flare loops. The density was found to increase at the rise of the impulsive peak, supporting chromospheric evaporation models. A notable difference is found in the surroundings of microflares; diffuse coronal jets are produced above microflares in coronal holes while coronal dimmings are formed in quiet regions. Conclusions. The microflares associated with bright points share common characteristics to active region flares. The difference in the surroundings of microflares are caused by open and closed configurations of the pre-existing magnetic field.

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“…These features are (a) the innermost part of the bubble, which is located at and around the center of the erupting field (marked by an asterisk), filled with dense plasma-we refer to this part as the "core" of the eruption, (b) the low-density area that immediately surrounds the "core"-we refer to this as the "cavity" and is the result of the cool adiabatic expansion of the rising magnetic field, and (c) the "front" of the erupting structure, which is a thin layer of dense material that envelops the "cavity" and demarcates the outskirts of the erupting field. To some extent, the shape of the eruptions in our simulations is reminiscent of the "three-part" structure of the observed small-scale prominence eruptions (mini or micro CMEs; e.g., Innes et al 2010;Raouafi et al 2010;Hong et al 2011) and/or CMEs (e.g., Reeves et al 2015). Because of this, we refer hereafter to the simulated eruptions as CME-like eruptions.…”

Section: Temperature Density Velocity and Currentmentioning

confidence: 87%

Recurrent CME-like Eruptions in Emerging Flux Regions. I. On the Mechanism of Eruptions

Syntelis

Archontis

Tsinganos

2017

ApJ

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We report on three-dimensional (3D) magnetohydrodynamic (MHD) simulations of recurrent eruptions in emerging flux regions. We find that reconnection of sheared field lines, along the polarity inversion line of an emerging bipolar region, leads to the formation of a new magnetic structure, which adopts the shape of a magnetic flux rope (FR) during its rising motion. Initially, the FR undergoes a slow-rise phase and, eventually, it experiences a fast-rise phase and ejective eruption toward the outer solar atmosphere. In total, four eruptions occur during the evolution of the system. For the first eruption, our analysis indicates that the torus instability initiates the eruption and that tether-cutting reconnection of the field lines, which envelop the FR, triggers the rapid acceleration of the eruptive field. For the following eruptions, we conjecture that it is the interplay between tether-cutting reconnection and torus instability that causes the onset of the various phases. We show the 3D shape of the erupting fields, focusing more on how magnetic field lines reconnect during the eruptions. We find that when the envelope field lines reconnect mainly with themselves, hot and dense plasma is transferred closer to the core of the erupting FR.The same area appears to be cooler and less dense when the envelope field lines reconnect with neighboring sheared field lines. The plasma density and temperature distribution, together with the rising speeds, energies, and size of the erupting fields, indicate that they may account for small-scale (mini) coronal mass ejections.

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STEREO quadrature observations of coronal dimming at the onset of mini-CMEs

Cited by 34 publications

References 12 publications

Oscillations in the wake of a flare blast wave

Oscillations in the wake of a flare blast wave

Evolution of microflares associated with bright points in coronal holes and in quiet regions

Recurrent CME-like Eruptions in Emerging Flux Regions. I. On the Mechanism of Eruptions

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